15
Summary Assembly of clusters of galaxies Assembly of clusters of galaxies * Large scale filamentary structures (>10Mpc) are seen in all clusters, providing good evidence for cluster scale assembly. * Large scale filamentary structures (>10Mpc) are seen in all clusters, providing good evidence for cluster scale assembly. Origins of morph-density/sfr-density relations Origins of morph-density/sfr-density relations * Truncation of SF is sharply seen in groups far out from cluster cores. * Truncation of SF is sharply seen in groups far out from cluster cores. * Truncation of SF and transformation of morphologies are driven by different physical processes (at least partly). * Truncation of SF and transformation of morphologies are driven by different physical processes (at least partly). Down-sizing in galaxy formation/evolution. Down-sizing in galaxy formation/evolution. * Massive galaxies form early while less massive galaxies (in final) form later or have more extended star formation. * Massive galaxies form early while less massive galaxies (in final) form later or have more extended star formation. * Down-sizing is a function of environment (=evolutionary stage). * Down-sizing is a function of environment (=evolutionary stage). high-density/high-mass  low-density/low-mass high-density/high-mass  low-density/low-mass